Figures REF  and REF  also suggest that the remnant radio galaxy is hosted by the 19.19 magnitude WISEA J152228.01\(+\) 274141.3 source that is 78 away from the optical galaxy V1CG 136 (R.A.: 15:22:28.5, decl.: \(+\) 27:41:46) at redshift \(z\)  = 0.072 [1]}. The cluster contains gas not only with an extremely wide range of temperatures and complex structure but that also shows a cold front at 30\(^{\prime \prime }\)  (\(\simeq \)  41.5 kpc) and a shock-like bow-shaped feature beyond \(\sim \) 100\(^{\prime \prime }\)  (\(\simeq \)  140 kpc) on the southeast of the southern cD [2]}. Figure REF  shows that the northeastern boundary of the remnant radio galaxy coincides with the 1.3 \(\times \)  10\(^{-7}\)  counts s\(^{-1}\)  arcsec\(^{-2}\)  surface-brightness contour level; gas in false color transitioning from the green region to the blue region at a distance of \(\sim \) 33\(^{\prime \prime }\)  (\(\simeq \)  45.7 kpc) from the southern cD galaxy.
All four panels of Figure REF  suggest that the radio emission from the remnant radio galaxy has an elongated, bar-shaped structure.
The remnant radio galaxy, buried in the radio halo emission that is barely detected using LOFAR at 153 MHz seems to possess an elongated, bar-shaped structure [3]}, consistent with our results.
This suggests that the remnant radio galaxy has a steep spectrum, and its consistency in radio morphology gives us additional confidence in our image fidelity, imaging, calibration and data reduction processes.
The best sensitivity image for the low surface-brightness was obtained from the 250–500 MHz band data and we now discuss below the morphology of the remnant radio galaxy.
